Molecular Gas Properties Under Icm Pressure in the Cluster Environment

Lee, Bumhyun; Chung, Aeree

doi:10.5303/pkas.2015.30.2.491

Cited by 2 publications

(3 citation statements)

References 23 publications

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“…Hence, using the Submillimeter Array (SMA) 1 , we have taken high-resolution 12CO (2−1) imaging data of a subsample of Virgo galaxies that have lost atomic gas significantly by ICM pressure. Some preliminary results are published in Lee & Chung (2015), and in this work, we present more complete analysis on both morphology and kinematics of three Virgo galaxies based on the SMA data.…”

Section: Introductionmentioning

confidence: 99%

The effect of ram pressure on the molecular gas of galaxies: three case studies in the Virgo cluster

Lee¹,

Chung²,

Tonnesen³

et al. 2016

Mon. Not. R. Astron. Soc.

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131

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We present 12CO (2-1) data of three Virgo spirals -NGC 4330, NGC 4402 and NGC 4522 obtained using the Submillimeter Array. These three galaxies show clear evidence of ram pressure stripping due to the cluster medium as found in previous HI imaging studies. Using high-resolution CO data, we investigate how the properties of the inner molecular gas disc change while a galaxy is undergoing HI stripping in the cluster. At given sensitivity limits, we do not find any clear signs of molecular gas stripping. However, both its morphology and kinematics appear to be quite disturbed as those of HI. Morphological peculiarities present in the molecular and atomic gas are closely related with each other, suggesting that molecular gas can be also affected by strong ICM pressure even if it is not stripped. CO is found to be modestly enhanced along the upstream sides in these galaxies, which may change the local star formation activity in the disc. Indeed, the distribution of Hα emission, a tracer of recent star formation, well coincides with that of the molecular gas, revealing enhancements near the local CO peak or along the CO compression. FUV and Hα share some properties in common, but FUV is always more extended than CO/Hα in the three galaxies, implying that the starforming disc is rapidly shrinking as the molecular gas properties have changed. We discuss how ICM pressure affects dense molecular gas and hence star formation properties while diffuse atomic gas is being removed from a galaxy.

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Section: Introductionmentioning

confidence: 99%

The effect of ram pressure on the molecular gas of galaxies: three case studies in the Virgo cluster

Lee¹,

Chung²,

Tonnesen³

et al. 2016

Mon. Not. R. Astron. Soc.

Self Cite

131

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“…The one-sided HI filaments are not always traced by close companions, such as NGC 4654 (Phookun & Mundy 1995), NGC 4330, NGC 4402, NGC 4522 and NGC 4569 in Virgo cluster (Chung et al 2009;Lee & Chung 2015). These galaxies appear to have head-tail shapes, with a compressed edge on one side and a long tail on the other side.…”

Section: Physical Properties Of the Galaxymentioning

confidence: 99%

“…A typical ram-pressure stripped HI morphology shows a headtail shape (Gavazzi et al 1995;van Gorkom et al 2003;Kenney et al 2004;Lee & Chung 2015). By mapping the HI gas distribution of galaxies in Virgo cluster, Chung et al (2009) found a remarkable number of galaxies with long, one-sided HI tails pointing away from M87, which were proposed to be the effect of ram-pressure stripping, in the sense that these galaxies are falling into the Virgo core for the first time.…”

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confidence: 99%

The Peculiar Filamentary H i Structure of NGC 6145

Wang

Kong

et al. 2017

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In this paper, we report the peculiar HI morphology of the cluster spiral galaxy NGC 6145, which has a 150 kpc HI filament on one side that is nearly parallel to its major axis. This filament is made up of several HI clouds and the diffuse HI gas between them, with no optical counterparts. We compare its HI distribution with other one-sided HI distributions in the literature, and find that the overall HI distribution is very different from the typical tidal and ram-pressure stripped HI shape, and its morphology is inconsistent with being a pure accretion event. Only ∼30% of the total HI gas is anchored on the stellar disk, while most of HI gas forms the filament in the west. At a projected distance of 122 kpc, we find a massive elliptical companion (NGC 6146) with extended radio emission, whose axis points to an HI gap in NGC 6145. The velocity of the HI filament shows an overall light-ofsight motion of 80 to 180 km s −1 with respect to NGC 6145. Using the long-slit spectra of NGC 6145 along its major stellar axis, we find that some outer regions show enhanced star formation, while in contrast, almost no star formation activities are found in its center (<2 kpc). Pure accretion, tidal or ram-pressure stripping is not likely to produce the observed HI filament. An alternative explanation is the jet-stripping from NGC 6146, although direct evidence for a jet-cold gas interaction has not been found.

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Molecular Gas Properties Under Icm Pressure in the Cluster Environment

Cited by 2 publications

References 23 publications

The effect of ram pressure on the molecular gas of galaxies: three case studies in the Virgo cluster

The effect of ram pressure on the molecular gas of galaxies: three case studies in the Virgo cluster

The Peculiar Filamentary H i Structure of NGC 6145

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